Anomalous HI in NGC 2997 and the Search for High Velocity Cloud Analogs

Astronomy and Astrophysics – Astronomy

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Scientific paper

We present the results of over 100 hours worth of HI observations of the isolated, inclined spiral galaxy, NGC 2997, to search for HI clouds analogous to the High Velocity Clouds (HVCs) seen around the Milky Way. After modeling a thin disk and fitting a rotation curve to the data, we characterize the left-over anomalous HI gas that contributes to 10% of the total HI emission. The HI line profiles of NGC 2997 show evidence for the existence of a "lagging disk": gas that is rotating in the same manner as the thin disk, but whose veloctiy decreases as a function of height from the disk. In fact, the majority of the anomalous gas in NGC 2997 may be associated with this sort of feature which has been previously detected in both HI and Halpha observations in edge-on spirals such as NGC 891, NGC 5775, NGC 4302 and the inclined NGC 2403. Simple ballistic models have tried to explain the lagging disk in the context of a galactic fountain (Shapiro & Field, 1976; Bregman, 1980). However, we also detect counter-rotating HI that does not appear to be associated with either the thin disk or the lagging disk. Just as in our own Milky Way, multiple processes, including accretion (Oort, 1966), may be necessary to explain the location of this high velocity HI.

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